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The CHANDRA data of the Classical Nova RR Pic (1925): A possible Magnetic Cataclysmic Variable Candidate

Published online by Cambridge University Press:  12 April 2016

Şölen Balman  and
Aybuke Küpcü-Yoldaş
Şölen Balman
Affiliation:
Middle East Technical University, Physics Dept., Inönü Bulvarn, Ankara, Turkey
Aybuke Küpcü-Yoldaş
Affiliation:
Middle East Technical University, Physics Dept., Inönü Bulvarn, Ankara, Turkey

Abstract

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During 25ksec of CHANDRA ACIS-S3 observations of the old nova RR Pic 1925 a count rate of 0.067±0.0017 c/s was detected. The results show evidence (spatial and spectral) for X-ray emission from the region around the prominent SW blob in the Hα images. Shell emission is detected with count rate ≥ (1.95±1.33)×10−3 c/s. The spectral analysis shows that the source spectrum can not be explained by a single or two temperature bremsstrahlung or VMEKAL models including photoelectric absorption, only models using powerlaw distribution of temperature fit the data well and indicate excess O, Al, Mg, S, and Si in the source spectrum. A soft excess in the CHANDRA data could be explained by a partial covering absorber model with covering fraction in a range 14-86 % consistent with characteristics of the Magnetic Cataclysmic Variable systems. The light curve shows significant orbital and other modulations.

Type
Part 3. A. Accretion Plasma diagnostics - Observations
Information
International Astronomical Union Colloquium , Volume 190: Magnetic Cataclysmic Variables , 2004 , pp. 172 - 173
Copyright
Copyright © Astronomical Society of the Pacific 2004

References

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